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  High angular resolution ALMA images of dust and molecules in the SN 1987A ejecta

Cigan, P., Matsuura, M., Gomez, H. L., Indebetouw, R., Abellán, F., Gabler, M., et al. (2019). High angular resolution ALMA images of dust and molecules in the SN 1987A ejecta. The Astrophysical Journal, 886(1): 51. doi:10.3847/1538-4357/ab4b46.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0005-A22D-2 Version Permalink: http://hdl.handle.net/21.11116/0000-0005-A22E-1
Genre: Journal Article

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 Creators:
Cigan, Phil, Author
Matsuura, Mikako, Author
Gomez, Haley L., Author
Indebetouw, Remy, Author
Abellán, Fran, Author
Gabler, Michael1, Author              
Richards, Anita, Author
Alp, Dennis, Author
Davis, Timothy A., Author
Janka, Hans-Thomas1, Author              
Spyromilio, Jason, Author
Barlow, M. J., Author
Burrows, David, Author
Dwek, Eli, Author
Fransson, Claes, Author
Gaensler, Bryan, Author
Larsson, Josefin, Author
Bouchet, P., Author
Lundqvist, Peter, Author
Marcaide, J. M., Author
Ng, C.-Y., AuthorPark, Sangwook, AuthorRoche, Pat, Authorvan Loon, Jacco Th., AuthorWheeler, J. C., AuthorZanardo, Giovanna, Author more..
Affiliations:
1Stellar Astrophysics, MPI for Astrophysics, Max Planck Society, ou_159882              

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 Abstract: We present high angular resolution (~80 mas) ALMA continuum images of the SN 1987A system, together with CO J=2 → 1, J=6 → 5, and SiO J=5 → 4 to J=7 → 6 images, which clearly resolve the ejecta (dust continuum and molecules) and ring (synchrotron continuum) components. Dust in the ejecta is asymmetric and clumpy, and overall the dust fills the spatial void seen in Hα images, filling that region with material from heavier elements. The dust clumps generally fill the space where CO J=6 → 5 is fainter, tentatively indicating that these dust clumps and CO are locationally and chemically linked. In these regions, carbonaceous dust grains might have formed after dissociation of CO. The dust grains would have cooled by radiation, and subsequent collisions of grains with gas would also cool the gas, suppressing the CO J=6 → 5 intensity. The data show a dust peak spatially coincident with the molecular hole seen in previous ALMA CO J=2 → 1 and SiO J=5 → 4 images. That dust peak, combined with CO and SiO line spectra, suggests that the dust and gas could be at higher temperatures than the surrounding material, though higher density cannot be totally excluded. One of the possibilities is that a compact source provides additional heat at that location. Fits to the far-infrared--millimeter spectral energy distribution give ejecta dust temperatures of 18--23K. We revise the ejecta dust mass to M<sub>dust</sub>=0.2−0.4M<sub>⊙</sub> for carbon or silicate grains, or a maximum of <0.7M<sub>⊙</sub> for a mixture of grain species, using the predicted nucleosynthesis yields as an upper limit.

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 Dates: 2019-11-19
 Publication Status: Published online
 Pages: -
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 Rev. Method: -
 Identifiers: DOI: 10.3847/1538-4357/ab4b46
Other: LOCALID: 3192639
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Title: The Astrophysical Journal
Source Genre: Journal
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Publ. Info: Bristol; Vienna : IOP Publishing; IAEA
Pages: - Volume / Issue: 886 (1) Sequence Number: 51 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_3